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Stellar Rotation and the Extended Main-Sequence Turnoff in the Open Cluster NGC 5822

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Stellar Rotation and the Extended Main-Sequence Turnoff in the Open Cluster NGC 5822 The Astrophysical Journal, 876:113 (9pp), 2019 May 10 https://doi.org/10.3847/1538-4357/ab16e4 © 2019. The American Astronomical Society. All rights reserved. Stellar Rotation and the Extended Main-sequence Turnoff in the Open Cluster NGC 5822 Weijia Sun1 , Richard de Grijs2,3 , Licai Deng4,5,6 , and Michael D. Albrow7 1 Kavli Institute for Astronomy & Astrophysics and Department of Astronomy, Peking University, Yi He Yuan Lu 5, Hai Dian District, Beijing 100871, Peopleʼs Republic of China 2 Department of Physics and Astronomy, Macquarie University, Balaclava Road, Sydney, NSW 2109, Australia 3 International Space Science Institute—Beijing, 1 Nanertiao, Hai Dian District, Beijing 100190, Peopleʼs Republic of China 4 Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, Peopleʼs Republic of China 5 School of Astronomy and Space Science, University of the Chinese Academy of Sciences, Huairou 101408, Peopleʼs Republic of China 6 Department of Astronomy, China West Normal University, Nanchong 637002, Peopleʼs Republic of China 7 School of Physical and Chemical Sciences, University of Canterbury, Private Bag 4800, Christchurch, New Zealand Received 2019 February 2; revised 2019 March 20; accepted 2019 April 6; published 2019 May 9 Abstract The origin of extended main-sequence turnoffs (eMSTOs) in intermediate-age (1–3 Gyr) clusters is one of the most intriguing questions in current star cluster research. Unlike the split main sequences found in some globular clusters, which are caused by bimodal populations in age and/or chemical abundances, eMSTOs are believed to be due to stellar rotation. We present a spectroscopic survey of MSTO stars in a nearby, intermediate-age (0.9 Gyr), 3 low-mass (∼1.7×10 Me) Galactic open cluster, NGC 5822. We derive a clean sample of member stars based on Gaia proper motions and parallaxes and confirm the existence of an eMSTO. Using medium-resolution (R∼4000) Southern African Large Telescope spectra, we derive the rotational velocities of 24 member stars (representing 20% completeness around the eMSTO region) and find that the loci of the main-sequence stars in the eMSTO region show a clear correlation with the projected rotational velocities in the sense that fast rotators are located on the red side of the eMSTO and slow rotators are found on the blue side. By comparison with a synthetic cluster model, we show that the stellar rotational velocities and the eMSTO of NGC 5822 can be well reproduced, and we conclude that stellar rotation is the main cause of the eMSTO in NGC 5822. Key words: galaxies: star clusters: general – open clusters and associations: individual (NGC 5822) – stars: rotation 1. Introduction Aided by Gaia Data Release 2 (DR2), we can derive “clean” The extended main-sequence turnoff (eMSTO) phenomenon samples of open clusters in the Milky Way free of contamina- tion by field stars (Cantat-Gaudin et al. 2018). The discovery of —i.e., the notion that the main-sequence turnoff (MSTO) in the eMSTOs in Galactic open clusters, similar to those observed in color–magnitude diagram (CMD) is much wider than the Magellanic Cloud clusters, has opened up a new chapter in our prediction from single stellar population modeling—first comprehension of the formation of eMSTOs and the evolution discovered in NGC 1846 by Mackey & Broby Nielsen of open clusters. Cordoni et al. (2018) found the existence of (2007), is a common feature found in a large fraction of eMSTOs in all 12 open clusters younger than ∼1.5 Gyr they young and intermediate-age (2 Gyr) massive Large and Small analyzed (including NGC 5822), suggesting that eMSTOs are a Magellanic Cloud clusters (e.g., Mackey et al. 2008; Milone common feature of intermediate-age clusters in the Milky Way et al. 2009, 2015; Goudfrooij et al. 2011; Li et al. 2014b; and that they are regulated by the same mechanism as that Correnti et al. 2017). operating in Magellanic Cloud clusters. The understanding of In the past few years, our understanding of the eMSTO open clusters, which used to be considered prototypes of a phenomenon in these clusters has been enriched and enhanced single stellar population, encountered a significant upheaval significantly. Rather than due to intrinsic age spreads, stellar due to the discovery of eMSTOs in Galactic open clusters. It rotation is believed to play an important role in shaping the has been reported that stars exhibit a wide range of rotation morphology of the eMSTO (e.g., Bastian & de Mink 2009;Li rates both in the field (Huang et al. 2010) and in open clusters et al. 2014a; Niederhofer et al. 2015). This theory is further (Huang & Gies 2006). A number of studies have explored the reinforced by multiple lines of photometric and spectroscopic effect of stellar rotation on the CMD around the MSTO region evidence. Using narrowband photometry, Bastian et al. (2017) (Brandt & Huang 2015a, 2015b, 2015c). However, the direct detected a large fraction (∼30%–60%) of Be stars in the MSTO connection between the stellar rotation rates of MSTO stars and regions of NGC 1850 (∼80 Myr) and NGC 1856 (∼280 Myr), their loci in the CMD was only revealed recently. Bastian et al. favoring the interpretation that their split main sequences are (2018) used Very Large Telescope/FLAMES spectroscopy of caused by the effects of fast rotators. Similar mechanisms were 60 cluster members in NGC 2818, an 800 Myr open cluster, to later confirmed in NGC 1866 (∼200 Myr) and NGC 1818 measure the stellar rotational velocities and found that stars (∼40 Myr) through high-resolution spectroscopic surveys, exhibiting high rotational velocities are located on the red side suggesting that these clusters host a blue main sequence of the eMSTO and those rotating slowly are on the blue side, in composed of slow rotators and a red one composed of fast agreement with the prediction of the stellar rotation scenario. rotators (Dupree et al. 2017; Marino et al. 2018b). Marino et al. (2018a) also reported that the multiple sequences 1 The Astrophysical Journal, 876:113 (9pp), 2019 May 10 Sun et al. Table 1 Observation Log of the SALT Runs Na ( ) ( ) Mask Name Program aJ2000 dJ2000 Exp. Time s Date UT (1)(2)(3)(4)(5)(6)(7) NGC5822p2 2017-2-SCI-038 15h04m33 43 −54°26′33 16 13 600 2018 Feb 8 2018-1-SCI-006 15h04m33 43 −54°26′33 16 13 764 2018 Aug 3 NGC5822p3 2017-2-SCI-038 15h04m19 43 −54°16′44 52 10 600 2018 Apr 26 NGC5822p4 2017-2-SCI-038 15h03m11 44 −54°16′22 93 11 600 2018 Feb 8 2018-1-SCI-006 15h03m11 44 −54°16′22 93 11 764 2018 Jul 30 NGC5822p6 2017-2-SCI-038 15h03m09 95 −54°31′46 39 9 600 2018 Feb 11 2018-1-SCI-006 15h03m09 95 −54°31′46 39 9 764 2018 Aug 14 NGC5822p8 2017-2-SCI-038 15h05m10 13 −54°19′41 91 7 600 2018 Feb 26 NGC5822p9 2017-2-SCI-038 15h04m36 35 −54°34′51 48 5 600 2018 Apr 30 Note. a Number of science slits in each field. they found in the young cluster NGC 6705 correspond to stellar of ∼4000 with a per-pixel resolution of 0.33 Å at a central populations with different rotation rates. wavelength of 4884.4 Å. Regular bias, argon arc lamp, and In this paper, we present a spectroscopic survey of MSTO quartz lamp flat-field calibration frames were taken as part of stars in the nearby (∼760 pc) intermediate-age (0.9 Gyr) open normal SALT operations. We used the PySALT package cluster NGC 5822. We find the presence of an eMSTO in this (Crawford et al. 2010) to perform the primary reduction and cluster and verify that it is not an artifact caused by differential wavelength calibration. For all of our samples, we obtained extinction. The loci of the main-sequence stars in the eMSTO spectra with a signal-to-noise ratio (S/N) per pixel in excess region show a clear correlation with the projected rotational of 200. velocities, with fast rotators lying on the red side of the eMSTO and slow rotators on the blue side. By comparison with a 2.2. Membership Determination synthetic cluster within the framework of stellar rotation, we Gaia ( argue that the observed morphology of the eMSTO in the CMD We exploited the DR2 Gaia Collaboration et al. ) can be properly explained by the model and that stellar rotation 2016, 2018 to analyze the stellar photometry, proper motions, is likely the main contributor to the eMSTO morphology in and parallaxes, and to perform membership determination in fi NGC 5822. the NGC 5822 eld. First, we acquired the stellar catalog from Gaia ( ′ This article is organized as follows. In Section 2 we present the database within 2.5 times the cluster radius 35 ; Dias ) the observations, data reduction procedures, and membership et al. 2002 . In the vector-point diagram of stellar proper motions, NGC 5822 showed a clear concentration centered at determination. Section 3 reports our main results, showing a -1 strong correlation between the stellar rotation rates and their (mqmadcos ,)(»- 7.44, - 5.52 ) mas yr . The other overden- -1 loci in the CMD region covered by the eMSTO. A discussion sity located at (mqmadcos ,)(»- 3.67, - 2.52 ) mas yr cor- and our conclusions are summarized in Section 4. responds to a nearby cluster, NGC 5823. Then, we derived the 22 quantity mR =-áñ+-áñ()()mqmqaacos cos mm ddand -1 2. Data Reduction and Analysis applied a cut of mR = 0.4 mas yr to conduct our primary 2.1.
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